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CNES activities in detectors for scientific space missions

CNES activities in detectors for scientific space missions. Alain BARDOUX a lain.bardoux@cnes.fr. SDW Florence 2013 – A Bardoux. CNES : French Space Agency. Helios, CSO Earth obs for Defence. SPOT, Pleiades Earth onservation. IASI, IASI-NG Atmospheric sounding. Gaia Star mapping.

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CNES activities in detectors for scientific space missions

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  1. CNES activities in detectors for scientific space missions Alain BARDOUX alain.bardoux@cnes.fr SDW Florence 2013 – A Bardoux 25/09/13 Réunion groupe Astro

  2. CNES : French Space Agency Helios, CSO Earth obs for Defence SPOT, Pleiades Earth onservation IASI, IASI-NG Atmospheric sounding Gaia Star mapping Corot Exoplanets Asterosismology And many others Herrschel Stars & Galaxies evolution Athena Black hole High energy astronomy B mode Origin of Univrse Exomars Mars Exploration Echo Exoplanets Microcarb CO2 survey SDW Florence 2013 – A Bardoux 25/09/13 Réunion groupe astro

  3. A travel through wavelengths …. and technologies Diamond QWIP CdTe Doped Si I-CCD NbSi MCT CCD CMOS InSb Tantal AlGaN Germanium TES InGaAs a-Si DSSD SDW Florence 2013 – A Bardoux

  4. X Ray SDW Florence 2013 – A Bardoux

  5. Missions In X ray domain • Missions in development • Taranis • SVOM • Solar Orbiter • Mission in pre-development (not decided) Athena (black holemattersurvey) Spectral domain 0.2-6keV (Instrument XMS, résolution 3eV@6keV) nominal solution based on TES (Goddard, NIST) Développement of an alternative solution Loft • French developemntsfocused on Front end ASIC’s SDW Florence 2013 – A Bardoux

  6. Xray microcalorimeter Detection of Xray photons Counting Energy measurement • Split of 3 functions • Absorbeur High Z • Sensor • Thermal insulation • + Specificelectronics DCT/SI/CD HG MAJ 12/10 SDW Florence 2013 – A Bardoux

  7. Xray microcalorimeter : on going development • Main axis • collective manufacturing • improvement of existing Technology (PACS) Silicon compatible technology • Goal • 32x32 demonstrateur for Athena • Technological choices • Absorbeur High Z Tantal • Sensor Doped Silicon • Thermal insulation SiO2 • Sensor temperature 50 to 70mK DCT/SI/CD HG MAJ 12/10 SDW Florence 2013 – A Bardoux

  8. Xray microcalorimeter Readout circuit Several stages to optimize thermal budget HEMT SiGe ASIC SDW Florence 2013 – A Bardoux

  9. Xray microcalorimeter : performances Signal : 30 to 100 µV/keV ie 150µV to 600 µV for a 6keV photon Energy range : 300 ev to 30 keV Dynamic : 300eV to 30keV ie 9µV to 3mV Noise Expected resolution : 6eV FWHM at 6 keV Noise 0,1µV to 0,3µV Power dissipation Goal 128 mW for 4000 pixels ie 1mW for 32 pixels DCT/SI/CD HG MAJ 12/10 SDW Florence 2013 – A Bardoux

  10. Xray microcalorimeter : realizations SDW Florence 2013 – A Bardoux

  11. Other activities in Xray domain Hybridation haute densité • LOFT :((IRAP) ultra low noise and consomption front end ASIC (15e ENC, 200µW) • Compton telescop : (APC) : tower of DSSD (soublestripped Si detector) up to 100MeV(See Youri Dolgorouky’s talk) • Germanium stripped detector (IRAP) ultimate performance spectro imager • (1 to 200keV) • CdTehighdensity focal plane (CEA/IRFU) : • small pixel (300µm) 4 sidebuttable module • for large and highdensity focal planes (reportés sur un support permettant de réduire la densité en face arrière) SDW Florence 2013 – A Bardoux

  12. Visible SDW Florence 2013 – A Bardoux

  13. Visible detection : CCD • No specificdeveloppment in terms of scientific detectors • CNES activityisfocused on High speed TDI for High resolutionpushbroomEarth observation (resolutionbelow 70cm) • Development of technogical blocks (at e2v) useful for future scientific detectors • Large wafer backthinned • Anti-etalonprocess • Black coating • Low noise on chip amplifier Close cooperationwith ESA SDW Florence 2013 – A Bardoux

  14. Visible Détection CMOS • No specificdeveloppment in terms of scientific detectors • CNES activityisfocused on High speed TDI for High resolutionpushbroomEarth observation (below 70cm) • sameconcern as ESA : setting up a wholesupplychainwhith good perennity • Design house • Foundry • backthinning • Assembly (spacequality) • Test and Space qualification • Developpment of technological blocks thatcouldbeuseful for scientific detectors • CCD on CMOS , allowing TDI detection and CMOS readout • Standard high performance »large » pixels (13 to 26µm pitch) • Qualification of µlens and commercial component • possible developpement for NEAT mission (Nearby Earth AstrometricTelescope) SDW Florence 2013 – A Bardoux

  15. To know more about CMOS detectors Workshop « CMOS for High Free registration at : https://cct.cnes.fr/content/workshop-cmos-image-sensors-high-performance-applications Or contact me alain.bardoux@cnes.fr SDW Florence 2013 – A Bardoux

  16. Infra Red SDW Florence 2013 – A Bardoux

  17. 2 main axis • Toward a large SWIR high performance detector (in coordination with ESA) • Toward a LWIR detector for Echo mission • Other activity • - Test of MCT APD SDW Florence 2013 – A Bardoux 25/09/13 Réunion groupe astro

  18. Large SWIR detectors Several activities • Improvement of manufacturing yield of large detectors • detection wafer size increasing, • hybridization reliability improvement • Development of a low noise readout circuit • Combined with a detection circuit impoved by ESA activity • -> prototype SDW Florence 2013 – A Bardoux 25/09/13 Réunion groupe astro

  19. high performance SWIR

  20. Echo mission • EChO (Exoplanet Characterisation Observatory; Cosmic Vision theme 1 - What are the conditions for planet formation and the emergence of life?) - a mission to investigate exoplanetary atmospheres, addressing the suitability of those planets for life and placing our Solar System in context Domain 5-12µm (French contribution) Driver : Dark current < 500é/s Technology : optimized HgCdTe • - SDW Florence 2013 – A Bardoux

  21. Developments for EChO • 4 detectors already fabricated and tested at CEA (LETI/Irfu) for temperature between 80 and 30K : • 1 detector fabricated with « standard » p/n technology • 3 detector fabricated with « optimisated » p/n technology • A large amount of pixels (on a detector) compliant with the need (< 500 e-/s) thanks to the optimised process. • Other wafer batch (p/n optimised process • at CEA Leti) under progress to provide 8 detectors to be tested by CEA Irfu SDW Florence 2013 – A Bardoux 25/09/13 Réunion groupe astro

  22. Submm & mm SDW Florence 2013 – A Bardoux

  23. Scientific missions in submm- mm • - Post Planck mission spectral domaine simililar to Plank one Planck (100, 143, 217, 353, 545 et 857 GHz ie, 350 µm to 3 mm) several technology candidate TES (NbSi) arrays LEKID arrays LETI all Solocon technology • Main drivers • Matrix development to improve performance and field of view • Collective manufacturing SDW Florence 2013 – A Bardoux

  24. TES • pixel has 3 main functions • Absorber (wavelength quarter cavity, antenna,…) • Senseur is a supra bolometer (TES) • Thermal insulation MUX à SQUID senseur TES SDW Florence 2013 – A Bardoux

  25. NbSi TES NEP~5.10-17 W/Hz 1/2 SDW Florence 2013 – A Bardoux

  26. LEKIDS (Lumped Element Kinetic Inductance Detectors ) • LEKID (Lumped element Kinetic Inductance Detector) is based on inductance variation of a supraconductor film wrt incident power : resonnant frequency variation • one metal layer on a silicon substrate • No MUX required ! DCT/SI/CD HG MAJ 12/10 SDW Florence 2013 – A Bardoux

  27. LEKID realization • a 144-pixel Aluminum array was fabricated and tested in a dilution fridge with optical access, yielding an average optical NEP of ~2E-16 W/Hz^1/2 (best pixels showed NEP = 6E-17 W/Hz^1/2 under 4-8 pW loading per pixel). • A second prototype of LEKIDs has been tested at the IRAM 30 m telescope. A new LEKID geometry for 2 polarizations will be presented. Also first optical measurements of a titanium nitride array. • Well asapted for 1mm-3mm range SDW Florence 2013 – A Bardoux

  28. Conclusion 25/09/13 Réunion groupe Astro

  29. Annunciation by Leonardo da Vinci Galleria degli Uffizi - Florence 25/09/13 Réunion groupe astro

  30. THANKS FOR YOUR ATTENTION 25/09/13 Réunion groupe astro

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